Medium resolution spectra of the dwarf nova BV Pup obtained during an outburst confirm the relatively long orbital period
( h). The emission lines reveal rather structured profiles that are produced
in the disc and in the stream. Doppler tomography shows clear bright spot regions in Hβ
and HeII 4686 Åemission line flux. Dynamical solutions for the system parameters are only
found if the external radius of the accretion disc is close to the circularisation radius.
The white dwarf mass is , the orbital inclination .

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